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Deep Very Large Telescope/MUSE optical integral field spectroscopy has recently revealed an abundant population of ultra-faint galaxies ( M _UV ≈ −15; 0.01 L _⋆ ) at z = 2.9−6.7 due to their strong Ly α emission with no detectable continuum. The implied Ly α equivalent widths can be in excess of 100–200 Å, challenging existing models of normal star formation and indicating extremely young ages, small stellar masses, and a very low amount of metal enrichment. We use JWST/NIRSpec’s microshutter array to follow up 45 of these galaxies (11 hr in G235M/F170LP and 7 hr in G395M/F290LP), as well as 45 lower-equivalent width Ly α emitters. Our spectroscopy covers the range 1.7−5.1 micron in order to target strong optical emission lines: H α , [O iii ], H β , and [N II]. Individual measurements as well as stacks reveal line ratios consistent with a metal-poor nature (2%−40% Z _⊙ , depending on the calibration). The galaxies with the highest equivalent widths of Ly α , in excess of 90 Å, have lower [N II]/H α (1.9 σ ) and [O iii ]/H β (2.2 σ ) ratios than those with lower equivalent widths, implying lower gas-phase metallicities at a combined significance of 2.4 σ . This implies a selection based on Ly α equivalent width is an efficient technique for identifying younger, less chemically enriched systems.