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Reliable models of the thermally pulsing asymptotic giant branch (TP-AGB)phase are of critical importance across astrophysics, including ourinterpretation of the spectral energy distribution of galaxies, cosmic dustproduction, and enrichment of the interstellar medium. With the aim ofimproving sets of stellar isochrones that include a detailed description of theTP-AGB phase, we extend our recent calibration of the AGB population in theSmall Magellanic Cloud (SMC) to the more metal rich Large Magellanic Cloud(LMC). We model the LMC stellar populations with the TRILEGAL code, using thespatially-resolved star formation history derived from the VISTA survey. Wecharacterize the efficiency of the third dredge-up by matching the star countsand the $K_{\rm s}$-band luminosity functions of the AGB stars identified inthe LMC. In line with previous findings, we confirm that, compared to the SMC,the third dredge-up in AGB stars of the LMC is somewhat less efficient, as aconsequence of the higher metallicity. The predicted range of initial mass ofC-rich stars is between $M_{\rm i} \approx 1.7 - 3~\mathrm{M}_{\odot}$ at$Z_{\rm i} = 0.008$. We show how the inclusion of new opacity data in thecarbon star spectra will improve the performance of our models. We discuss thepredicted lifetimes, integrated luminosities and mass-loss rate distributionsof the calibrated models. The results of our calibration are included inupdated stellar isochrones publicly available.

Constraining the thermally pulsing asymptotic giant branch phase with resolved stellar populations in the Large Magellanic Cloud