We present the spatially resolved star formation history (SFH) of a shell-like structure located in the northeastern Small Magellanic Cloud (SMC). We quantitatively obtain the SFH using unprecedented deep photometric data (g ∼ 24 magnitude) from the SMASH survey and colour-magnitude diagram (CMD) fitting techniques. We consider, for the first time, the SMC's line-of-sight depth and its optical effects on the CMDs. The SFH presents higher accuracy when a line-of-sight depth of ∼ 3 kpc is simulated. We find young star formation enhancements at ∼150 Myr, ∼200 Myr, ∼450 Myr, ∼650 Myr, and ∼1 Gyr. Comparing the structure's SFH with the Large Magellanic Cloud's northern arm SFH we show strong evidence of synchronicity from at least the past ∼2.8 Gyr, possibly ∼3.5 Gyr. Our results place constraints on the orbital history of the Magellanic Clouds which, potentially, have implications on their dynamical mass estimates.