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We present results from the first application of the Grid of Red Supergiantand Asymptotic Giant Branch ModelS (GRAMS) model grid to the entire evolvedstellar population of the Large Magellanic Cloud (LMC). GRAMS is a pre-computedgrid of 80,843 radiative transfer (RT) models of evolved stars andcircumstellar dust shells composed of either silicate or carbonaceous dust. Wefit GRAMS models to ~30,000 Asymptotic Giant Branch (AGB) and Red Supergiant(RSG) stars in the LMC, using 12 bands of photometry from the optical to themid-infrared. Our published dataset consists of thousands of evolved stars withindividually determined evolutionary parameters such as luminosity andmass-loss rate. The GRAMS grid has a greater than 80% accuracy ratediscriminating between Oxygen- and Carbon-rich chemistry. The global dustinjection rate to the interstellar medium (ISM) of the LMC from RSGs and AGBstars is on the order of 1.5x10^(-5) solar masses/yr, equivalent to a totalmass injection rate (including the gas) into the ISM of ~5x10^(-3) solarmasses/yr. Carbon stars inject two and a half times as much dust into the ISMas do O-rich AGB stars, but the same amount of mass. We determine a bolometriccorrection factor for C-rich AGB stars in the K band as a function of J - Kcolor, BC(K) = -0.40(J-K)^2 + 1.83(J-K) + 1.29. We determine several IR colorproxies for the dust mass-loss rate (MLR) from C-rich AGB stars, such as log(MLR) = (-18.90)/((K-[8.0])+3.37)-5.93. We find that a larger fraction of AGBstars exhibiting the `long-secondary period' phenomenon are O-rich than starsdominated by radial pulsations, and AGB stars without detectable mass-loss donot appear on either the first-overtone or fundamental-mode pulsationsequences.

The Mass-Loss Return From Evolved Stars to The Large Magellanic Cloud VI: Luminosities and Mass-Loss Rates on Population Scales