  Stellar-mass black holes (BHs) can be retained in globular clusters (GCs)
until the present. Simulations of GC evolution find that the relaxation driven
mass-loss rate is elevated if BHs are present, especially near dissolution. We
capture this behaviour in a parameterised mass-loss rate, benchmarked by
results from $N$-body simulations, and use it to evolve an initial GC mass
function (GCMF), similar to that of young massive clusters in the Local
Universe, to an age of 12 Gyr. Low-metallicity GCs ([Fe/H]$\lesssim-1.5$) have
the highest mass-loss rates, because of their relatively high BH masses, which
combined with their more radial orbits and stronger tidal field in the past
explains the high turnover mass of the GCMF ($\sim10^5\,{\rm M}_\odot$) at
large Galactic radii ($\gtrsim 10\,$kpc). The turnover mass at smaller Galactic
radii is similar as the result of the upper mass truncation of the initial GCMF
and the lower mass-loss rate because of the higher metallicities. The density
profile in the Galaxy of mass lost from massive GCs ($\gtrsim10^{5}\,{\rm
M}_\odot$) resembles that of nitrogen-rich stars in the halo, confirming that
these stars originated from GCs. We conclude that two-body relaxation is the
dominant effect in shaping the GCMF from a universal initial GCMF, because
including the effect of BHs reduces the need for additional disruption
mechanisms.
