We present optical, near-infrared, and radio observations of supernova (SN) SN IIb 2022crv. We show that it retained a very thin H envelope and transitioned from an SN IIb to an SN Ib; prominent H{alpha} seen in the pre-maximum phase diminishes toward the post-maximum phase, while HeI lines show increasing strength. SYNAPPS modeling of the early spectra of SN 2022crv suggests that the absorption feature at 6200{AA} is explained by a substantial contribution of H{alpha} together with SiII, as is also supported by the velocity evolution of H{alpha}. The light-curve evolution is consistent with the canonical stripped-envelope SN subclass but among the slowest. The light curve lacks the initial cooling phase and shows a bright main peak (peak M_V_=-17.82{\pm}0.17mag), mostly driven by radioactive decay of ^56^Ni. The light-curve analysis suggests a thin outer H envelope (Menv~0.05M_{sun}) and a compact progenitor (Renv~3R{sun}). An interaction-powered synchrotron self-absorption model can reproduce the radio light curves with a mean shock velocity of 0.1c. The mass-loss rate is estimated to be in the range of (1.9-2.8)x10^-5^M{sun}_/yr for an assumed wind velocity of 1000km/s, which is on the high end in comparison with other compact SNe IIb/Ib. SN 2022crv fills a previously unoccupied parameter space of a very compact progenitor, representing a beautiful continuity between the compact and extended progenitor scenario of SNe IIb/Ib.