We present the first spatially resolved study of molecular gas in the vicinity of a Gamma Ray Burst , using CO ( 2-1 ) emission line observations with the Atacama Large Millimetre Array ( ALMA ) at \sim 50 pc scales . The host galaxy of GRB 980425 contains a ring of high column density H i gas which is likely to have formed due to a collision between the GRB host and its companion galaxy , within which the GRB is located . We detect eleven molecular gas clumps in the galaxy , seven of which are within the gas ring . The clump closest to the GRB position is at a projected separation of \sim 280 pc . Although it is plausible that the GRB progenitor was ejected from clusters formed in this clump , we argue that the in situ formation of the GRB progenitor is the most likely scenario . We measure the molecular gas masses of the clumps and find them to be sufficient for forming massive star clusters . The molecular gas depletion times of the clumps show a variation of \sim 2 dex , comparable with the large variation in depletion times found in starburst galaxies in the nearby Universe . This demonstrates the presence of starburst modes of star formation on local scales in the galaxy , even while the galaxy as a whole can not be categorised as a starburst based on its global properties . Our findings suggest that the progenitor of GRB 9802425 was originated in a young massive star cluster formed in the starburst mode of star formation .