[Abridged] Tight correlations between supermassive black hole (SMBH) mass
($M_{\rm BH}$) and the properties of the host galaxy have useful implications
for our understanding of the growth of SMBHs and evolution of galaxies. Here,
we present newly observed correlations between $M_{\rm BH}$ and the host galaxy
total UV$-$ [3.6] color ($\mathcal{C_{\rm UV,tot}}$, Pearson's r = $0.6-0.7$)
for a sample of 67 galaxies (20 early-type galaxies and 47 late-type galaxies)
with directly measured $M_{\rm BH}$ in the GALEX/S$^{4}$G survey. The colors
are carefully measured in a homogeneous manner using the galaxies' FUV, NUV and
3.6 $\micron$ magnitudes and their multi-component structural decompositions in
the literature. We find that more massive SMBHs are hosted by (early- and
late-type) galaxies with redder colors, but the $M_{\rm BH}- \mathcal{C_{\rm
UV,tot}}$ relations for the two morphological types have slopes that differ at
$\sim 2 \sigma$ level. Early-type galaxies define a red sequence in the $M_{\rm
BH}- \mathcal{C_{\rm UV,tot}}$ diagrams, while late-type galaxies trace a blue
sequence. Within the assumption that the specific star formation rate of a
galaxy (sSFR) is well traced by $L_{\rm UV}/L_{\rm 3.6}$, it follows that the
SMBH masses for late-type galaxies exhibit a steeper dependence on sSFR than
those for early-type galaxies. The $M_{\rm BH}- \mathcal{C_{\rm UV,tot}}$ and
$M_{\rm BH}-L_{\rm 3.6,tot}$ relations for the sample galaxies reveal a
comparable level of vertical scatter in the log $M_{\rm BH}$ direction, roughly
$5\%-27\%$ more than the vertical scatter of the $M_{\rm BH}-\sigma$ relation.
Our $M_{\rm BH}- \mathcal{C_{\rm UV,tot}}$ relations suggest different channels
of SMBH growth for early- and late-type galaxies, consistent with their
distinct formation and evolution scenarios.