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We present results from a study of the distances and distribution of a sampleof intermediate-age clusters in the Large Magellanic Cloud. Using deepnear-infrared photometry obtained with ISPI on the CTIO 4m, we have measuredthe apparent K-band magnitude of the core helium burning red clump stars in 17LMC clusters. We combine cluster ages and metallicities with the work ofGrocholski & Sarajedini to predict each cluster's absolute K-band red clumpmagnitude, and thereby calculate absolute cluster distances. An analysis ofthese data shows that the cluster distribution is in good agreement with thethick, inclined disk geometry of the LMC, as defined by its field stars. Wealso find that the old globular clusters follow the same distribution,suggesting that the LMC's disk formed at about the same time as the globularclusters, ~ 13 Gyr ago. Finally, we have used our cluster distances inconjunction with the disk geometry to calculate the distance to the LMC center,for which we find (m-M)o = 18.40 +/- 0.04_{ran} +/- 0.08_{sys}, or Do = 47.9+/- 0.9 +/- 1.8 kpc.

Distances to Populous Clusters in the LMC via the K-Band Luminosity of the Red Clump