We combine VI photometry from OGLE-III with VVV and 2MASS measurements of E ( J - K _ { s } ) to resolve the longstanding problem of the non-standard optical extinction toward the Galactic bulge . We show that the extinction is well-fit by the relation A _ { I } = 0.7465 { \times } E ( V - I ) +1.3700 { \times } E ( J - K _ { s } ) , or , equivalently , A _ { I } = 1.217 { \times } E ( V - I ) ( 1 + 1.126 { \times } ( E ( J - K _ { s } ) / E ( V - I ) -0.3433 ) ) . The optical and near-IR reddening law toward the inner Galaxy approximately follows an R _ { V } \approx 2.5 extinction curve with a dispersion { \sigma } _ { R _ { V } } \approx 0.2 , consistent with extragalactic investigations of the hosts of type Ia SNe . Differential reddening is shown to be significant on scales as small as as our mean field size of 6 \arcmin . The intrinsic luminosity parameters of the Galactic bulge red clump ( RC ) are derived to be ( M _ { I,RC } , \sigma _ { I,RC, 0 } , ( V - I ) _ { RC, 0 } , \sigma _ { ( V - I ) _ { RC } } , ( J - K _ { s } ) _ { RC, 0 } ) = ( % -0.12 , 0.09 , 1.06 , 0.121 ,\ 0.66 ) . Our measurements of the RC brightness , brightness dispersion and number counts allow us to estimate several Galactic bulge structural parameters . We estimate a distance to the Galactic center of 8.20 kpc . We measure an upper bound on the tilt \alpha \approx 40 ^ { \circ } between the bulge ’ s major axis and the Sun-Galactic center line of sight , though our brightness peaks are consistent with predictions of an N-body model oriented at \alpha \approx 25 ^ { \circ } . The number of RC stars suggests a total stellar mass for the Galactic bulge of \sim 2.3 { \times } 10 ^ { 10 } M _ { \odot } if one assumes a canonical Salpeter IMF , or \sim 1.6 { \times } 10 ^ { 10 } M _ { \odot } if one assumes a bottom-light Zoccali IMF .