  We investigate potential correlations between radio source counts (after
background corrections) of 22 Galactic globular clusters (GCs) from the MAVERIC
survey, and stellar encounter rates ($\Gamma$) and masses ($M$) of the GCs.
Applying a radio luminosity limit of $L_\mathrm{lim}=5.0\times
10^{27}~\mathrm{erg~s^{-1}}$, we take a census of radio sources in the core and
those within the half-light radius. By following a maximum likelihood method
and adopting a simplified linear model, we find an unambiguous dependence of
core radio source counts on $\Gamma$ and/or $M$ at 90% confidence, but no clear
dependence of source counts within the half-light radius on either $\Gamma$ or
$M$. Five of the identified radio sources in cores above our adopted limit are
millisecond pulsars or neutron star X-ray binaries (XRBs), the dependence of
which on $\Gamma$ is well-known, but another is a published black hole (BH) XRB
candidate, and ten others are not identified. Accounting for the verified
cluster members increases the significance of correlation with $M$ and/or
$\Gamma$ (to 99% confidence), for fits to core and half-light region source
counts, while excluding a dependence on $\Gamma$ alone at 90% (core) and 68%
(half-light) confidence. This is consistent with published dynamical
simulations of GC BH interactions that argue $\Gamma$ will be a poor predictor
of the distribution of accreting BHs in GCs. Future multiwavelength follow-up
to verify cluster membership will enable stronger constraints on the dependence
of radio source classes on cluster properties, promising a new view on the
dynamics of BHs in GCs.
