Studying Relation Between Star Formation and Molecular Clumps on Subparsec Scales in 30 Doradus

We present ${}^{12}\mathrm{C}\mathrm{O}$ and ${}^{13}\mathrm{C}\mathrm{O}$ molecular gas data observed by ALMA, massive early stage young stellar objects identified by applying color-magnitude cuts to $\mathit{\text{Spitzer}}$ and $\mathit{\text{Herschel}}$ photometry, and low-mass late stage young stellar objects identified via H$\alpha$ excess. Using dendrograms, we derive properties for the molecular cloud structures. This is the first time a dendrogram analysis has been applied to extragalactic clouds. The majority of clumps have a virial parameter equal to unity or less. The size-linewidth relations of ${}^{12}\mathrm{C}\mathrm{O}$ and ${}^{13}\mathrm{C}\mathrm{O}$ show the clumps in this study have a larger linewidth for a given size (by factor of 3.8 and 2.5, respectively) in comparison to several, but not all, previous studies. The larger linewidths in 30 Doradus compared to typical Milky Way quiescent clumps are probably due to the highly energetic environmental conditions of 30 Doradus. The slope of the size-linewidth relations of ${}^{12}\mathrm{C}\mathrm{O}$, 0.65 $\pm$ 0.04, and ${}^{13}\mathrm{C}\mathrm{O}$, 0.97 $\pm$ 0.12, are on the higher end but consistent within 3$\sigma$ of previous studies. Massive star formation occurs in clumps with high masses ($>1.83\times {10}^2{\mathrm{M}}_{\odot }$), high linewidths (v $>1.18\mathrm{k}\mathrm{m}\mathrm{/}\mathrm{s}$), and high mass densities ($> 6.67 \times 10^{2};${\mathrm{M}}_{\odot }\mathrm{p}{\mathrm{c}}^{-2}$$). The majority of embedded, massive young stellar objects are associated with a clump. However the majority of more evolved, low-mass young stellar objects are not associated with a clump.