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This study aims at identifying and understanding the parent population ofnovae in the Large Magellanic Cloud (LMC) by studying the local, projected,stellar population. The star formation history of the local environment aroundnovae is studied based on photometric data of stars and star clusters in thenova neighbourhood, available in the OGLE II survey and star clustercatalogues. The ages of stellar population within a few arcmin around novaeregions are estimated using isochrone fits to the V vs (V-I) colour-magnitudediagrams. The fraction of stars in various evolutionary states are comparedusing luminosity functions of the main-sequence stars and the red giant stars.The age, density and luminosity function of the stellar population areestimated around 15 novae. The upper limit of the age of the intermediatestellar population is found to be 4 Gyr in all the regions, excepting theregion around the slow nova LMC 1948. Star formation in these regions is foundto have started between 4 - 2.0 Gyr, with a majority of the regions startingthe star formation at 3.2 Gyr. This star formation event lasted until 1.6 - 0.8Gyr The star formation history of the underlying population of both the fastand moderately fast novae indicate their parent population to be similar andlikely to be in the age range 3.2 - 1.0 Gyr. This is in good agreement with thetheoretical age estimates for Galactic cataclysmic variables. The region aroundthe slow nova shows a stellar population in the age range 1 - 10 Gyr, with agood fraction belonging to an older population, consistent with the idea thatthe progenitors of slow novae belong to older population.Comment: to appear in A&A (final version - error analysis included, typos  corrected, figures 17 and 18 changed

The local stellar population of nova regions in the Large Magellanic Cloud