Abstract
The author discusses the main properties of the family of star clusters in the Large Magellanic Cloud (LMC). To this aim, he first reviews the stellar models for low and intermediate mass stars in occurrence of convective overshoot, and then describes an algorithm suitable for a theoretical approach to cluster photometry (colour magnitude C-M) diagrams, luminosity functions (LF), integrated magnitudes and colours, and total masses). The Johnson B-V CCD photometry of the stellar content of NGC 1866 is presented and used to test the theoretical models for intermediate mass stars with convective overshoot. The conclusion of this analysis is that these models fit the C-M diagram and LF of NGC 1866 much better than any other type of models in the literature. In addition to this, the Johnson B-V CCD photometry of NGC 1831, another populous cluster of LMC, is presented and analyzed by means of the same stellar models. The author also presents new estimates of the total mass of many clusters derived from their integrated B-V magnitudes. Finally a few words are addressed to the issue of the history of star formation in the field stars of LMC.
