We present the first measurement of the spatial clustering of mid-infrared selected obscured and unobscured quasars , using a sample in the redshift range 0.7 < z < 1.8 selected from the 9 deg ^ { 2 } Boötes multiwavelength survey . Recently the Spitzer Space Telescope and X-ray observations have revealed large populations of obscured quasars that have been inferred from models of the X-ray background and supermassive black hole evolution . To date , little is known about obscured quasar clustering , which allows us to measure the masses of their host dark matter halos and explore their role in the cosmic evolution of black holes and galaxies . In this study we use a sample of 806 mid-infrared selected quasars and \approx 250,000 galaxies to calculate the projected quasar-galaxy cross-correlation function w _ { p } ( R ) . The observed clustering yields characteristic dark matter halo masses of \log ( M _ { halo } [ h ^ { -1 } M _ { \sun } ] ) = 12.7 ^ { +0.4 } _ { -0.6 } and 13.3 ^ { +0.3 } _ { -0.4 } for unobscured quasars ( QSO-1s ) and obscured quasars ( Obs-QSOs ) , respectively . The results for QSO-1s are in excellent agreement with previous measurements for optically-selected quasars , while we conclude that the Obs-QSOs are at least as strongly clustered as the QSO-1s . We test for the effects of photometric redshift errors on the optically-faint Obs-QSOs , and find that our method yields a robust lower limit on the clustering ; photo- z errors may cause us to underestimate the clustering amplitude of the Obs-QSOs by at most \sim 20 % . We compare our results to previous studies , and speculate on physical implications of stronger clustering for obscured quasars .