Abstract
We present the galaxy cluster autocorrelation function of 277 galaxy cluster candidates with 0.25 ⩽ z ⩽ 1.5 in a 7 deg2 area of the IRAC Shallow Cluster Survey. We find strong clustering throughout our galaxy cluster sample, as expected for these massive structures. Specifically, at ⟨z⟩ = 0.5 we find a correlation length of 
Mpc, in excellent agreement with the Las Campanas Distant Cluster Survey, the only other nonlocal measurement. At higher redshift, ⟨z⟩ = 1, we find that strong clustering persists, with a correlation length of 
Mpc. A comparison with high-resolution cosmological simulations indicates these are clusters with halo masses of ~1014 M☉, a result supported by estimates of dynamical mass for a subset of the sample. In a stable clustering picture, these clusters will evolve into massive (1015 M☉) clusters by the present day.
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