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Context: Grids of stellar models, computed with the same physicalingredients, allow one to study the impact of a given physics on a broad rangeof initial conditions and are a key ingredient for modeling the evolution ofgalaxies. Aims: We present a grid of single star models for masses between 0.8and 120 $M_\odot$, with and without rotation for a mass fraction of heavyelement Z=0.006, representative of the Large Magellanic Cloud (LMC). Methods:We used the Geneva stellar evolution code. The evolution was computed until theend of the central carbon-burning phase, the early asymptotic giant branchphase, or the core helium-flash for massive, intermediate, and low mass stars,respectively. Results: The outputs of the present stellar models are wellframed by the outputs of the two grids obtained by our group for metallicitiesabove and below the one considered here. The models of the present work providea good fit to the nitrogen surface enrichments observed during the mainsequence for stars in the LMC with initial masses around 15 $M_\odot$. Theyalso reproduce the slope of the luminosity function of red supergiants of theLMC well, which is a feature that is sensitive to the time-averaged mass lossrate over the red supergiant phase. The most massive black hole that can beformed from the present models at Z=0.006 is around 55 $M_\odot$. No model inthe range of mass considered will enter into the pair-instability supernovaregime, while the minimal mass to enter the region of pair pulsationinstability is around 60 $M_\odot$ for the rotating models and 85 $M_\odot$ forthe nonrotating ones. Conclusions: The present models are of particularinterest for comparisons with observations in the LMC and also in the outerregions of the Milky Way. We provide public access to numerical tables that canbe used for computing interpolated tracks and for population synthesis studies.

Grids of stellar models with rotation VI: Models from 0.8 to 120 $M_\odot$ at a metallicity Z = 0.006