  Gravitational waves (GW) can be employed as standard sirens that will soon
measure the Hubble constant with sufficient precision to weigh in on the $\sim
5\sigma$ Hubble tension. Most GW sources will have no identified
electromagnetic counterpart, leading to uncertainty in the redshift of the
source, and in turn a degeneracy between host galaxy distance, redshift, and
$H_0$. In the case where no electromagnetic counterparts are identified, it has
been proposed that a statistical canvassing of candidate GW hosts, found in a
large galaxy survey for example, can be used to accurately constrain the Hubble
constant. We study and simulate this "galaxy voting" method to compute $H_0$.
We find that the Hubble constant posterior is in general biased relative to the
true value even when making optimistic assumptions about the statistical
properties of the sample. Using the MICECAT light-cone catalog, we find that
the bias in the $H_0$ posteriors depends on the realization of the underlying
galaxy sample and the precision of the GW source distance measurement.
