  We identify cosmic voids from galaxy density fields under the theory of
void-cluster correspondence. We extend the previous novel void-identification
method developed for the matter density field to the galaxy density field for
practical applications. From cosmological N-body simulations, we construct
galaxy number- and mass-weighted density fields to identify cosmic voids that
are counterparts of galaxy clusters of specific mass. The parameters for the
cluster-counterpart void identification such as Gaussian smoothing scale,
density threshold, and core volume fraction are found for galaxy density
fields. We achieve about $60$--$67\%$ of completeness and reliability for
identifying the voids of corresponding cluster mass above
$3\times10^{14}h^{-1}M_{\odot}$ from a galaxy sample with the mean number
density, $\bar{n}=4.4\times10^{-3} (h^{-1}{\rm Mpc})^{-3}$. When the mean
density is increased to $\bar{n}=10^{-2} (h^{-1}{\rm Mpc})^{-3}$, the detection
rate is enhanced by $\sim2$--$7\%$ depending on the `mass scale' of voids. We
find that the detectability is insensitive to the density weighting scheme
applied to generate the density field. Our result demonstrates that we can
apply this method to the galaxy redshift survey data to identify cosmic voids
corresponding statistically to the galaxy clusters in a given mass range.
