We investigate the kinematic properties of the Coma galaxy cluster using a new, large, spectroscopic sample of member galaxies, from the Dark Energy Spectroscopic Instrument (DESI). By means of the MG-MAMPOSST code, which is based on the Jeans equation, we jointly reconstruct the total cluster mass profile and the velocity anisotropy profile. Assuming a Navarro-Frenk-White model, we estimate a virial mass of M200c=1.04^+0.07^-0.08(stat)+/-0.09(syst)x10^15^M_{sun}, corresponding to r200c=2.07+/-0.05Mpc and a scale radius for the mass profile of rs=0.73^+0.30^-0.24_ (stat) +/- 0.21 (syst) Mpc, which provides the tightest robust kinematic mass profile constraint to date. By separately considering the mass of the hot gas and the galaxy stellar mass, we further determined the dark matter mass profile, with M200c^DM^=8.6^+1.2^-0.8_x10^14^M{sun}_. We discuss the impact of the mass and galaxy number density parametrisations, the effect induced by different choices of the cluster's rest frame and of the radial range of the kinematic analysis, further comparing our results with previous estimates from the literature. The cluster dynamical state was also assessed, using the spatial and line-of-sight velocity distributions of the members. We also analysed the line-of-sight velocity distributions and anisotropy profiles of different galaxy populations, selected based on their colour (red sequence, green valley, and blue cloud). The orbits of green valley and blue cloud galaxies appear to be more radial in the centre and in the outskirts, respectively, with the latter predicting a higher cluster virial mass. This study provides new insights into the interplay between dynamical and intrinsic properties of galaxies in massive structures, which is fundamental to verify the tight connection between a galaxy's evolution and its environment.

Cone search capability for table J/A+A/710/A218/table4 (Galaxy before magnitude cut)