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We simulate the formation of a low metallicity (0.01 Zsun) stellar cluster ina dwarf galaxy at redshift z~14. Beginning with cosmological initialconditions, the simulation utilizes adaptive mesh refinement and sink particlesto follow the collapse and evolution of gas past the opacity limit forfragmentation, thus resolving the formation of individual protostellar cores. Atime- and location-dependent protostellar radiation field, which heats the gasby absorption on dust, is computed by integration of protostellar evolutionarytracks with the MESA code. The simulation also includes a robustnon-equilibrium chemical network that self-consistently treats gasthermodynamics and dust-gas coupling. The system is evolved for 18 kyr afterthe first protostellar source has formed. In this time span, 30 sink particlesrepresenting protostellar cores form with a total mass of 81 Msun. Their massesrange from ~0.1 Msun to 14.4 Msun with a median mass ~0.5-1 Msun. Massiveprotostars grow by competitive accretion while lower-mass protostars arestunted in growth by close encounters and many-body ejections. In the regimeexplored here, the characteristic mass scale is determined by the temperaturefloor set by the cosmic microwave background and by the onset of efficientdust-gas coupling. It seems unlikely that host galaxies of the first bursts ofmetal-enriched star formation will be detectable with the James Webb SpaceTelescope or other next-generation infrared observatories. Instead, the mostpromising access route to the dawn of cosmic star formation may lie in thescrutiny of metal-poor, ancient stellar populations in the Galacticneighborhood. The observable targets that correspond to the system simulatedhere are ultra-faint dwarf satellite galaxies such as Bootes II, Segue I andII, and Willman I.

Star formation in the first galaxies - III. Formation, evolution, and characteristics of the first stellar cluster