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We present high-spatial-resolution ($\sim 0\farcs2$, or $\sim$3\,pc) CO(2--1)observations of the nearest young starburst dwarf galaxy, NGC\,5253, taken withthe Atacama Large Millimeter/submillimeter Array. We have identified 118molecular clouds with average values of 4.3\,pc in radius and 2.2\,\kms\, invelocity dispersion, which comprise the molecular cloud complexes observedpreviously with $\sim$100\,pc resolution. We derive for the first time in thisgalaxy the $I{\rm (CO)}$--$N$(H$_2$) conversion factor, $X$ =$4.1^{+5.9}_{-2.4}\times10^{20}$\,cm$^{-2}$(K\,\kms)$^{-1}$, based on thevirial method. The line-width and mass-to-size relations of the resolvedmolecular clouds present an offset on average toward higher line-widths andmasses with respect to quiescent regions in other nearby spiral galaxies andour Galaxy. The offset in the scaling relation reaches its maximum in regionsclose to the central starburst, where velocity dispersions are $\sim$ 0.5 dexhigher and gas mass surface densities are as high as $\Sigma_{\rm H_2}$ =10$^3$\,\Msol\,pc $^{-2}$. These central clouds are gravitationally bounddespite the high internal pressure. A spatial comparison with star clustersfound in the literature enables us to identify six clouds that are associatedwith young star clusters. Furthermore, the star formation efficiencies (SFEs)of some of these clouds exceed those found in star-cluster-forming cloudswithin our Galaxy. We conclude that once a super star cluster is formed, theparent molecular clouds are rapidly dispersed by the destructive stellarfeedback, which results in such a high SFE in the central starburst ofNGC\,5253.

ALMA Observations toward the starburst dwarf galaxy NGC 5253: I. Molecular cloud properties and scaling relations