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We derive the mass-radius relation and mass function of molecular clumps inthe Large Magellanic Cloud (LMC) and interpret them in terms of the simplefeedback model proposed by Fall, Krumholz, and Matzner (FKM). Our work utilizesthe dendrogram-based catalog of clumps compiled by Wong et al. from $^{12}$COand $^{13}$CO maps of six giant molecular clouds in the LMC observed with theAtacama Large Millimeter Array (ALMA). The Magellanic Clouds are the onlyexternal galaxies for which this type of analysis is possible at the necessaryspatial resolution ($\sim1$ pc). We find that the mass-radius relation and massfunction of LMC clumps have power-law forms, $R \propto M^{\alpha}$ and $dN/dM\propto M^{\beta}$, with indices $\alpha = 0.36 \pm 0.03$ and $\beta= -1.8 \pm0.1 $ over the mass ranges $10^2 M_\odot \lesssim M \lesssim 10^5 M_\odot$ and$10^2 M_\odot \lesssim M \lesssim 10^4 M_\odot$, respectively. With thesevalues of $\alpha$ and $\beta$ for the clumps (i.e., protoclusters), thepredicted index for the mass function of young LMC clusters from the FKM modelis $\beta \approx 1.7$, in good agreement with the observed index. Thesituation portrayed here for clumps and clusters in the LMC replicates that inthe Milky Way.

Feedback in Forming Star Clusters: The Mass-Radius Relation and Mass Function of Molecular Clumps in the Large Magellanic Cloud