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We present near-infrared spectroscopy of the host galaxy of dark GRB 080325using Subaru/MOIRCS. The obtained spectrum provides a clear detection ofH$\alpha$ emission and marginal [NII]$\lambda$6584. The host is a massive(M$_{*}\sim10^{11}$M$_{\odot}$), dusty ($A_{V}\sim 1.2$) star-forming galaxy atz=1.78. The star formation rate calculated from the H$\alpha$ luminosity(35.6-47.0 M$_{\odot}$ yr$^{-1}$) is typical among GRB host galaxies (andstar-forming galaxies generally) at z $>$1; however, the specific starformation rate is lower than normal star-forming galaxies at redshift $\sim$1.6, in contrast to the high specific star formation rates measured for many ofother GRB hosts. The metallicity of the host is estimated to be12+log(O/H)$_{\rm KK04}$$=$8.88. We emphasize that this is one of the mostmassive distant host galaxies for which metallcity is measured withemission-line diagnostics. The metallicity is fairly high among GRB hosts.However, this is still lower than the metallicity of normal star-forminggalaxies of the same mass at z$\sim$1.6. The metallicity offset from normalstar-forming galaxies is close to a typical value of other GRB hosts andindicates that GRB host galaxies are uniformly biased toward low metalicityover a wide range of redshift and stellar mass. The low-metallicity nature ofthe GRB 080325 host is likely not attributable to the fundamental metallicityrelation of star-forming galaxies beacuse it is a metal-poor outlier from therelation and has a low sSFR. Thus we conclude that metallicity is important tothe mechanism that produced this GRB.

The Redshift and Metallicity of the Host Galaxy of Dark GRB 080325 at z=1.78