Planets form during the first few Myr of the evolution of the star-disk system, possibly before the end of the embedded phase. The properties of very young disks and their subsequent evolution reflect the presence and properties of their planetary content. We present a study of the Class II/F disk population in L1688, the densest and youngest region of star formation in Ophiuchus. We also compare it to other well-known nearby regions of different ages, namely Lupus, Chamaeleon I, Corona Australis, Taurus and Upper Scorpius. We selected our L1688 sample using a combination of criteria (available ALMA data, Gaia membership, and optical and near-IR spectroscopy) to determine the stellar and disk properties, specifically stellar mass (M), average population age, mass accretion rate (dM/dt_acc_) and disk dust mass (Mdust). We applied the same procedure in a consistent manner to the other regions. Results. In L1688 the relations between dM/dt_acc_ and M, Mdust and M, and dM/dt_acc_ Mdust have a roughly linear trend with slopes 1.8-1.9 for the first two relations and ~1 for the third, which is similar to what found in the other regions. When ordered according to the characteristic age of each region, which ranging from ~0.5 to ~5Myr, dM/dt_acc_ as t^-1^, when corrected for the different stellar mass content; Mdust follows roughly the same trend, ranging between 0.5 and 5Myr, but has an increase of a factor of ~3 at ages of 2-3Myr. We suggest that this could result from an earlier planet formation, followed by collisional fragmentation that temporarily replenishes the millimeter-size grain population. The dispersion of dM/dt_acc_ and Mdust around the best-fitting relation with M, as well as that of dM/dt_acc_ Mdust are equally large. When adding all the regions together to increase the statistical significance, we find that the dispersions have continuous distributions with a log-normal shape and similar widths (~0.8dex). This detailed study of L1688 confirms the general picture of Class II/F disk properties and extends it to a younger age. The amount of dust observed at ~1Myr is not sufficient to assemble the majority of planetary systems, which suggests an earlier formation process for planetary cores. The dust mass traces to a large extent the disk gas mass evolution, even if the ratio Mdust/Mdisk at the earliest age (0.5-1Myr) is not known. Two properties are still not understood: the steep dependence of dM/dt_acc_ Mdust on M* and the cause of the large dispersion in the three relations analyzed in this paper, in particular that of the dM/dt_acc_ Mdust relation.

Cone search capability for table J/A+A/663/A98/tablea1 (VLMS and BDs in L1688 with ALMA 0.89mm data)

Cone search capability for table J/A+A/663/A98/tableb1 (Properties of stars and disks in L1688)

Cone search capability for table J/A+A/663/A98/tablec1 (Properties of stars and disks in Lupus)

Cone search capability for table J/A+A/663/A98/tabled1 (Properties of stars and disks in Upper Scorpius)

Cone search capability for table J/A+A/663/A98/tablee1 (Properties of stars and disks in Chamaeleon I)

Cone search capability for table J/A+A/663/A98/tablef1 (Properties of stars and disks in Corona Australis)

Cone search capability for table J/A+A/663/A98/tableg1 (Properties of stars and disks in Taurus)