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We present the mass-metallicity relation (MZR) for a parent sample of 604galaxies at $z=5.34-6.94$ with [\text{O}~\textsc{iii}] doublets detected, usingthe deep JWST/NIRCam wide field slitless spectroscopic (WFSS) observations in26 quasar fields. The sample incorporates the full observations of 25 quasarfields from JWST Cycle 1 GO program ASPIRE and the quasar SDSS J0100+2802 fromJWST EIGER program. We identify 204 galaxies residing in overdense structuresusing friends-of-friends (FoF) algorithm. We estimate the electron temperatureof $2.0^{+0.3}_{-0.4}\times10^4$ K from the Hg and$[\text{O}~\textsc{iii}]_{4363}$ lines in the stacked spectrum, indicating ametal-poor sample with median gas phase metallicity12+$\log(\mathrm{O/H})=7.64^{+0.23}_{-0.11}$. With the most up-to-date strongline calibration based on NIRSpec observations, we find that the MZR shows ametal enhancement of $\sim0.2$ dex at high mass end in overdense environments.However, compared to the local Fundamental Metallicity Relation (FMR), ourgalaxy sample at $z>5$ shows a metal deficiency of $\sim0.2$ dex relative toFMR predictions. We explain the observed trend of FMR with a simple analyticalmodel, and we favor dilution from intense gas accretion over outflow to explainthe metallicity properties at $z>5$. Those high redshift galaxies are likely ina rapid gas accretion phase when their metal and gas contents are in anon-equilibrium state. According to model predictions, the protocluster membersare closer to the gas equilibrium state than field galaxies and thus havehigher metallicity and are closer to the local FMR. Our results suggest thatthe accelerated star formation during protocluster assembly likely plays a keyrole in shaping the observed MZR and FMR, indicating a potentially earlieronset of metal enrichment in overdense environments at $z\approx5-7$.

Insights on Metal Enrichment and Environmental Effect at $z\approx5-7$ with JWST ASPIRE/EIGER and Chemical Evolution Model