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[en] We spectroscopically survey the galaxy cluster XMM-LSS J02182-05102 (hereafter IRC 0218) using LRIS (optical) and MOSFIRE (near-infrared) on Keck I as part of the ZFIRE survey. IRC 0218 has a narrow redshift range of defined by 33 members of which 20 are at R Mpc. The cluster redshift and velocity dispersion are and km s−1. We reach NIR line sensitivities of ∼0.3 × 10−17 erg s−1 cm−2 that, combined with multi-wavelength photometry, provide extinction-corrected Hα star formation rates (SFR), gas phase metallicities from [N ii]/Hα, and stellar masses. We measure an integrated Hα SFR of ∼325 (26 members; R Mpc) and show that the elevated star formation in the cluster core (R Mpc) is driven by the concentration of star-forming members, but the average SFR per Hα-detected galaxy is half that of members at R ∼ 1 Mpc. However, we do not detect any environmental imprint when comparing attenuation and gas phase metallicities: the cluster galaxies show similar trends with as to the field, e.g., more massive galaxies have larger stellar attenuation. IRC 0218’s gas phase metallicity– relation (MZR) is offset to lower metallicities relative to and has a slope of 0.13 ± 0.10. Comparing the MZR in IRC 0218 to the COSMOS cluster at z = 2.1 shows no evolution ( Gyr): the MZR for both galaxy clusters are remarkably consistent with each other and virtually identical to several field surveys at .