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In order to precisely determine temperature and density of molecular gas inthe Large Magellanic Cloud, we made observations of optically thin$^{13}$CO($J=3-2$) transition by using the ASTE 10m telescope toward 9 peakswhere $^{12}$CO($J=3-2$) clumps were previously detected with the sametelescope. The molecular clumps include those in giant molecular cloud (GMC)Types I (with no signs of massive star formation), II (with HII regions only),and III (with HII regions and young star clusters). We detected$^{13}$CO($J=3-2$) emission toward all the peaks and found that theirintensities are 3 -- 12 times lower than those of $^{12}$CO($J=3-2$). Wedetermined the intensity ratios of $^{12}$CO($J=3-2$) to $^{13}$CO($J=3-2$),$R^{12/13}_{3-2}$, and $^{13}$CO($J=3-2$) to $^{13}$CO($J=1-0$),$R^{13}_{3-2/1-0}$, at 45$\arcsec$ resolution. These ratios were used forradiative transfer calculations in order to estimate temperature and density ofthe clumps. The parameters of these clumps range kinetic temperature$T\mathrm{_{kin}}$ = 15 -- 200 K, and molecular hydrogen gas density$n(\mathrm{H_2})$ = 8$\times 10^2$ -- 7$\times 10^3$ cm$^{-3}$. We confirmedthat the higher density clumps show higher kinetic temperature and that thelower density clumps lower kinetic temperature at a better accuracy than in theprevious work. The kinetic temperature and density increase generally from aType I GMC to a Type III GMC. We interpret that this difference reflects anevolutionary trend of star formation in molecular clumps. The$R^{13}_{3-2/1-0}$ and kinetic temperature of the clumps are well correlatedwith H$\alpha$ flux, suggesting that the heating of molecular gas$n(\mathrm{H_2})$ = $10^3$ -- $10^4$ cm$^{-3}$ can be explained by stellar FUVphotons.

Dense Clumps in Giant Molecular Clouds in the Large Magellanic Cloud: Density and Temperature Derived from $^{13}$CO($J=3-2$) Observations