  The origin of the black hole mergers detected by LIGO and Virgo remains an
open question. While the unusual mass and spin of a few events constrain their
possible astrophysical formation mechanisms, it is difficult to classify the
bulk of the observed mergers. Here we consider the distribution of masses and
spins in LIGO/Virgo's first and second observing catalogs, and find that for a
significant fraction (25%) of these detected events, an AGN-disk origin model
is preferred over a parametric mass-spin model fit to the full GWTC-2 merger
sample (Bayes factor $\mathcal{B}>10$). We use this to estimate the black hole
merger rate in AGNs to be about $2.8\pm 1.8$\, Gpc$^{-3}$yr$^{-1}$, comparable
to theoretical expectations. We find that AGNs can explain the rate and mass
distribution of the observed events with primary black hole mass in the
pair-instability mass gap ($M\gtrsim50$\, M$_\odot$).
