  Using 3.6$\mu$m images of 97 early-type galaxies, we develop and verify
methodology to measure globular cluster populations from the S$^4$G survey
images. We find that 1) the ratio, T$_{\rm N}$, of the number of clusters,
N$_{\rm CL}$, to parent galaxy stellar mass, M$_*$, rises weakly with M$_*$ for
early-type galaxies with M$_* > 10^{10}$ M$_\odot$ when we calculate galaxy
masses using a universal stellar initial mass function (IMF), but that the
dependence of T$_{\rm N}$ on M$_*$ is removed entirely once we correct for the
recently uncovered systematic variation of IMF with M$_*$, and 2) for M$_* <
10^{10}$ M$_\odot$ there is no trend between N$_{\rm CL}$ and M$_*$, the
scatter in T$_{\rm N}$ is significantly larger (approaching 2 orders of
magnitude), and there is evidence to support a previous, independent suggestion
of two families of galaxies. The behavior of N$_{\rm CL}$ in the lower mass
systems is more difficult to measure because these systems are inherently
cluster poor, but our results may add to previous evidence that large
variations in cluster formation and destruction efficiencies are to be found
among low mass galaxies. The average fraction of stellar mass in clusters is
$\sim$ 0.0014 for M$_* > 10^{10}$ M$_\odot$ and can be as large as $\sim 0.02$
for less massive galaxies. These are the first results from the S$^4$G sample
of galaxies, and will be enhanced by the sample of early-type galaxies now
being added to S$^4$G and complemented by the study of later type galaxies
within S$^4$G.
