We report the discovery of a super-damped Lyman-alpha absorber at $z_{abs}=2.2068$ toward QSO Q1135-0010 in the Sloan Digital Sky Survey, and follow-up VLT UVES spectroscopy. Voigt profile fit to the DLA line indicates log $N_{rm H I} = 22.05 pm 0.1$. This is the second QSO DLA discovered to date with such high $N_{rm H I}$. We derive element abundances [Si/H] = $-1.10 pm 0.10$, [Zn/H] = $-1.06 pm 0.10$, [Cr/H] = $-1.55 pm 0.10$, [Ni/H] = $-1.60 pm 0.10$, [Fe/H] = $-1.76 pm 0.10$, [Ti/H] = $-1.69 pm 0.11$, [P/H] = $-0.93 pm 0.23$, and [Cu/H] = $-0.75 pm 0.14$. Our data indicate detection of Ly-$alpha$ emission in the DLA trough, implying a star formation rate of $sim$10 $M_{odot}$ yr$^{-1}$ in the absence of dust attenuation. C II$^{*} , lambda 1336$ absorption is also detected, suggesting SFR surface density $-2 < {rm log} , dot{psi_{*}} < 0$ $M_{odot}$ yr$^{-1}$ kpc$^{-2}$. We estimate electron density in the range $3.5 times 10^{-4}$ to 24.7 cm$^{-3}$ from C II$^{*}$/C II, and $sim$0.5-0.9 cm$^{-3}$ from Si II$^{*}$/Si II. Overall, this is a robustly star-forming, moderately enriched absorber, but with relatively low dust depletion. Fitting of the SDSS spectrum yields low reddening for Milky Way, LMC, or SMC extinction curves. No CO absorption is detected, and C I absorption is weak. The low dust and molecular content, reminiscent of some SMC sight-lines, may result from the lower metallicity, and a stronger radiation field (due to higher SFR). Finally, we compare this absorber with other QSO and GRB DLAs.
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