The first discovery of the gravitational-wave ( GW ) event , GW150914 , suggests a higher merger rate of black-hole ( BH ) binaries . If this is true , a number of BH binaries will be observed via the second-generation GW detectors , and the statistical properties of the observed BH binaries can be scrutinized . A naive but important question to ask is whether the spatial distribution of BH binaries faithfully traces the matter inhomogeneities in the Universe or not . Although the BH binaries are thought to be formed inside the galaxies in most of the scenarios , there is no observational evidence to confirm such a hypothesis . Here , we estimate how well the second-generation GW detectors can statistically confirm the BH binaries to be a tracer of the large-scale structure by looking at the auto- and cross-correlation of BH binaries with photometric galaxies and weak-lensing measurements , finding that , with a 3 year observation , the > 3 \sigma detection of a non-zero signal is possible if the BH merger rate today is \dot { n } _ { 0 } \gtrsim 100 Gpc ^ { -3 } yr ^ { -1 } and the clustering bias of BH binaries is b _ { BH, 0 } \gtrsim 1.5 .