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Simulations predict that the galaxy populations inhabiting protoclusters maycontribute considerably to the total amount of stellar mass growth of galaxiesin the early universe. In this study, we test these predictionsobservationally, focusing on the Taralay protocluster (formerly PCl J1001+0220)at $z \sim 4.57$ in the COSMOS field. Leveraging data from the Charting ClusterConstruction with VUDS and ORELSE (C3VO) survey, we spectroscopically confirmed44 galaxies within the adopted redshift range of the protocluster ($4.48 < z <4.64$) and incorporate an additional 18 such galaxies from ancillaryspectroscopic surveys. Using a density mapping technique, we estimate the totalmass of Taralay to be $\sim 1.7 \times 10^{15}$ M$_\odot$, sufficient to form amassive cluster by the present day. By comparing the star formation ratedensity (SFRD) within the protocluster (SFRD$_\text{pc}$) to that of the coevalfield (SFRD$_\text{field}$), we find that SFRD$_\text{pc}$ surpasses theSFRD$_\text{field}$ by $\Delta$log(SFRD/$M_\odot$ yr$^{-1}$ Mpc$^{-3}$) = $1.08\pm 0.32$ (or $\sim$ 12$\times$). The observed contribution fraction ofprotoclusters to the cosmic SFRD adopting Taralay as a proxy for typicalprotoclusters is $33.5\%^{+8.0\%}_{-4.3\%}$, a value $\sim$2$\sigma$ in excessof the predictions from simulations. Taralay contains three peaks that are$5\sigma$ above the average density at these redshifts. Their SFRD is $\sim$0.5dex higher than the value derived for the overall protocluster. We show that68% of all star formation in the protocluster takes place within these peaks,and that the innermost regions of the peaks encase $\sim 50\%$ of the totalstar formation in the protocluster. This study strongly suggests thatprotoclusters drive stellar mass growth in the early universe and that thisgrowth may proceed in an inside-out manner.

Protoclusters as Drivers of Stellar Mass Growth in the Early Universe, a Case Study: Taralay -- a Massive Protocluster at z ~ 4.57