  We present results from a study of the globular cluster luminosity function
(GCLF) in a sample of 89 early-type galaxies observed as part of the ACS Virgo
Cluster Survey. Using a Gaussian parametrization of the GCLF, we find a highly
significant correlation between the GCLF dispersion, sigma, and the galaxy
luminosity, M_B, in the sense that the GC systems in fainter galaxies have
narrower luminosity functions. The GCLF dispersions in the Milky Way and M31
are fully consistent with this trend, implying that the correlation between
sigma and galaxy luminosity is more fundamental than older suggestions that
GCLF shape is a function of galaxy Hubble type. We show that the sigma - M_B
relation results from a bonafide narrowing of the distribution of (logarithmic)
cluster masses in fainter galaxies. We further show that this behavior is
mirrored by a steepening of the GC mass function for relatively high masses, M
>~ 3 x 10^5 M_sun, a mass regime in which the shape of the GCLF is not strongly
affected by dynamical evolution over a Hubble time. We argue that this trend
arises from variations in initial conditions and requires explanation by
theories of cluster formation. Finally, we confirm that in bright galaxies, the
GCLF "turns over" at the canonical mass scale of M_TO ~ 2 x 10^5 M_sun.
However, we find that M_TO scatters to lower values (~1-2 x 10^5 M_sun) in
galaxies fainter than M_B >~ -18.5, an important consideration if the GCLF is
to be used as a distance indicator for dwarf ellipticals.
