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Applying dendrogram analysis to the CARMA-NRO C$^{18}$O ($J$=1--0) datahaving an angular resolution of $\sim$ 8", we identified 692 dense cores in theOrion Nebula Cluster (ONC) region. Using this core sample, we compare the coreand initial stellar mass functions in the same area to quantify the step fromcores to stars. About 22 \% of the identified cores are gravitationally bound.The derived core mass function (CMF) for starless cores has a slope similar toSalpeter's stellar initial mass function (IMF) for the mass range above 1$M_\odot$, consistent with previous studies. Our CMF has a peak at a subsolarmass of $\sim$ 0.1 $M_\odot$, which is comparable to the peak mass of the IMFderived in the same area. We also find that the current star formation rate isconsistent with the picture in which stars are born only from self-gravitatingstarless cores. However, the cores must gain additional gas from thesurroundings to reproduce the current IMF (e.g., its slope and peak mass),because the core mass cannot be accreted onto the star with a 100\% efficiency.Thus, the mass accretion from the surroundings may play a crucial role indetermining the final stellar masses of stars.

The Core Mass Function in the Orion Nebula Cluster Region: What Determines the Final Stellar Masses?