Based on photometric observations made with the CTIO “Victor Blanco” 4m telescope, we present the results of a study of the chemical evolution of the Large Magellanic Cloud (LMC) for the last 2.2 Gyr. As tracers of the LMC chemical enrichment, we used 39 star clusters projected on the bar, 27 on the inner disc and 15 on the outer disc. Our sample includes 44 previously unstudied clusters. In all cases we determined size, reddening, deprojected distance, age and metallicity. We show that the more metal-rich clusters are mainly located in the inner disc, while more metalpoor clusters are distributed throughout the entire disc. Intermediate-age clusters ten to be located at greater deprojected galactocentric distances while the youngest ones are mainly found in the inner disc. These trends are maintained when the sample is complemented with clusters observed by other authors with the same technique. These results reinforce the idea of the absence of a radial metallicity gradient in the LMC for clusters with subsolar metallicities. The resulting age-metallicity relationship appears to be independent of which LMC region is considered.