  Recent studies suggest that globular clusters (GCs) may retain a substantial
population of stellar-mass black holes (BHs), in contrast to the long-held
belief of a few to zero BHs. We model the population of BH low-mass X-ray
binaries (BH-LMXBs), an ideal observable proxy for elusive single BHs, produced
from a representative group of Milky Way GCs with variable BH populations. We
simulate the formation of BH-binaries in GCs through exchange interactions
between binary and single stars in the company of tens to hundreds of BHs.
Additionally, we consider the impact of the BH population on the rate of
compact binaries undergoing gravitational wave driven mergers. The
characteristics of the BH-LMXB population and binary properties are sensitive
to the GCs structural parameters as well as its unobservable BH population. We
find that GCs retaining $\sim 1000$ BHs produce a galactic population of $\sim
150$ ejected BH-LMXBs whereas GCs retaining only $\sim20$ BHs produce zero
ejected BH-LMXBs. Moreover, we explore the possibility that some of the
presently known BH-LMXBs might have originated in GCs and identify five
candidate systems.
