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The zero point of the reddening toward the Large Magellanic Cloud (LMC) hasbeen the subject of some dispute. Its uncertainty propagates as a systematicerror for methods which measure the extragalactic distance scale throughknowledge of the absolute extinction of LMC stars. In an effort to resolve thisissue, we used three different methods to calibrate the most widely-used metricto predict LMC extinction, the intrinsic color of the red clump,$(V-I)_{RC,0}$, for the inner $\sim$3 degrees of that galaxy. The firstapproach was to empirically calibrate the color zeropoints of the BaSTIisochrones over a wide metallicity range of ${\Delta}\rm{[Fe/H]} \approx 1.10$using measurements of red clump stars in 47 Tuc, the Solar Neighborhood, andNGC 6791.  From these efforts we also measure these properties of the Solar Neighborhoodred clump, ($V-I$, $G_{BP}-K_{s}$, $G-K_{s}$, $G_{RP}-K_{s}$, $J-K_{s}$,$H-K_{s}$, $M_{I}$, $M_{Ks}$)$_{RC,0} =$ (1.02, 2.75, 2.18, 1.52, 0.64, 0.15,$-$0.23, $-$1.63). The second and third methods were to compare the observedcolors of the red clump to those of Cepheids and RR Lyrae in the LMC. Withthese three methods, we estimated the intrinsic color of the red clump of theLMC to be $(V-I)_{RC,0,\rm{LMC}} = \{ \approx 0.93,0.91 \pm 0.02,0.89 \pm0.02\}$ respectively, and similarly using the first and third method weestimated $ (V-I)_{RC,0,\rm{SMC}} = \{\approx 0.85,0.84 \pm 0.02 \}$respectively for the Small Magellanic Cloud. We estimate the luminosities to be$M_{I,RC,\rm{LMC}}=-0.26$ and $M_{I,RC,\rm{SMC}}=-0.37$. We show that this hasimportant implications for recent calibrations of the tip of the red giantbranch in the Magellanic Clouds used to measure $H_0$.

On the Color-Metallicity Relation of the Red Clump and the Reddening Toward the Magellanic Clouds