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We analyzed HST/WFPC2 colour-magnitude diagrams (CMDs) of 15 populous LargeMagellanic Cloud (LMC) stellar clusters with ages between ~ 0.3 Gyr and ~ 3Gyr. These (V, B-V) CMDs are photometrically homogeneous and typically reach V\~ 22. Accurate and self-consistent physical parameters (age, metallicity,distance modulus and reddening) were extracted for each cluster by comparingthe observed CMDs with synthetic ones. These determinations involvedsimultaneous statistical comparisons of the main-sequence fiducial line and thered clump position, offering objective and robust criteria to determine thebest models. The models explored a regular grid in the parameter space coveredby previous results found in the literature. In general, the best models show asatisfactory fit to the data, constraining well the physical parameters of eachcluster. The age-metallicity relation derived by us presents a lower spreadthan similar results found in the literature for the same clusters. Our resultsare in accordance with the published ages for the oldest clusters, but reveal apossible underestimation of ages by previous authors for the youngest clusters.Our metallicity results in general agree with the ones based on spectroscopy ofgiant stars and with recent works involving CMD analyses. The derived distancemoduli implied by the most reliable solutions, correlate with the reddeningvalues, as expected from the non-negligible three-dimensional distribution ofthe clusters within the LMC. The inferred spatial distribution for theseclusters is roughly aligned with the LMC disk, being also more scattered thanrecent numerical predictions, indicating that they were not formed in the LMCdisk. The set of ages and metallicities homogeneously derived here can be usedto calibrate integrated light studies applied to distant galaxies.Comment: 20 pages, 35 Postscript figures, A&A, accepted 03 October 200

Physical parameters of 15 intermediate-age LMC clusters from modelling of HST colour–magnitude diagrams