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We use deep \textit{Hubble Space Telescope} spectroscopy to constrain themetallicities and (\editone{light-weighted}) ages of massive ($\logM_\ast/M_\odot\gtrsim10$) galaxies selected to have quiescent stellarpopulations at $1.0<z<1.8$. The data include 12--orbit depth coverage with theWFC3/G102 grism covering $\sim$ $8,000<\lambda<11,500$~\AA\, at a spectralresolution of $R\sim 210$ taken as part of the CANDELS Lyman-$\alpha$ Emissionat Reionization (CLEAR) survey. At $1.0<z<1.8$, the spectra cover importantstellar population features in the rest-frame optical. We simulate a suite ofstellar population models at the grism resolution, fit these to the data foreach galaxy, and derive posterior likelihood distributions for metallicity andage. We stack the posteriors for subgroups of galaxies in different redshiftranges that include different combinations of stellar absorption features. Ourresults give \editone{light-weighted ages of $t_{z \sim 1.1}= 3.2\pm 0.7$~Gyr,$t_{z \sim 1.2}= 2.2\pm 0.6$~Gyr, $t_{z\sim1.3}= 3.1\pm 0.6$~Gyr, and$t_{z\sim1.6}= 2.0 \pm 0.6$~Gyr, \editone{for galaxies at $z\sim 1.1$, 1.2,1.3, and 1.6. This} implies that most of the massive quiescent galaxies at$1<z<1.8$ had formed $>68$\% of their stellar mass by a redshift of $z>2$}. Theposteriors give metallicities of \editone{$Z_{z\sim1.1}=1.16 \pm0.29$~$Z_\odot$, $Z_{z\sim1.2}=1.05 \pm 0.34$~$Z_\odot$, $Z_{z\sim1.3}=1.00 \pm0.31$~$Z_\odot$, and $Z_{z\sim1.6}=0.95 \pm 0.39$~$Z_\odot$}. This is evidencethat massive galaxies had enriched rapidly to approximately Solar metallicitiesas early as $z\sim3$.

CLEAR I: Ages and Metallicities of Quiescent Galaxies at $\mathbf{1.0 < z < 1.8}$ Derived from Deep Hubble Space Telescope Grism Data