We report millimeter/submillimeter continuum and molecular line observations of the Galactic super star cluster RCW 38, obtained from the Atacama Large Millimeter/Submillimeter Array with a minimum angular resolution of $0.17times0.15$ ($simeq289,{rm AU}times255,{rm AU}$). The C$^{18}$O image reveal many massive condensations embedded within filamentary structures extending along the northwest-southeast direction in the center of cluster. The condensations have sizes of 0.01-0.02 pc, H$_2$ column densities of $10^{23}$-$10^{24}$ cm$^{-2}$, and H$_2$ masses of 10-130 $M_odot$. In addition, the 233-GHz continuum image reveals two dense, small millimeter-sources with radii of 460 and 200 AU (Source A and Source B). Source A is embedded within the most massive C$^{18}$O condensation, whereas no counterpart is seen for Source B. The masses of Source A and Source B are estimated as 13 and 3 $M_odot$ at the optically-thin limit, respectively. The C$^{18}$O emission shows a velocity gradient of 2 km s$^{-1}$ at the central 2000 AU of Source A, which could be interpreted as a Keplerian rotation with a central mass of a few $M_odot$ or infall motion of gas. Further, the ALMA $^{12}$CO data reveal that Source A and Source B are associated with molecular outflows exhibiting maximum velocities of $sim$30-70 km s$^{-1}$. The outflows have short dynamical timescales of $<$1000 yr and high mass outflow rates of $sim10^{-4}$-$10^{-3}$ $M_odot$ yr$^{-1}$. These observational signatures suggest an early evolutionary phase of the massive star formation in Source A and Source B.
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