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-N, of the number of clusters, N-CL, to parent galaxy stellar mass, M-*, rises weakly with M-* for early-type galaxies with M-* > 10(10) M-circle dot when we calculate galaxy masses using a universal stellar initial mass function (IMF) but that the dependence of T-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-circle dot, there is no trend between N-CL and M-*, the scatter in T-N is significantly larger (approaching two orders of magnitude), and there is evidence to support a previous, independent suggestion of two families of galaxies. The behavior of N-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 similar to 0.0014 for M-* > 10(10) M-circle dot and can be as large as similar to 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.