  The recent detection of gravitational waves from a binary merger involving a
potential low-mass gap black hole (LMBH) by LIGO-Virgo-KAGRA (LVK)
Collaboration motivates investigations into mechanisms beyond conventional
stellar evolution theories to account for their existence. We study a mechanism
in which dark matter (DM), through its capture and accumulation inside main
sequence stars, induces the formation of black holes within the mass range of
$[3, 5]M_\odot$. We examine the distribution of these LMBHs as a function of
galaxy halo mass, particularly when paired with neutron stars. This gives a
distinct signature that can be tested with future gravitational wave
observations. We find that a viable portion of the DM parameter space predicts
a merger rate of such binaries consistent with LVK observations.
