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Cluster formation and gas dynamics in the central regions of barred galaxiesare not well understood. This paper reviews the environment of three 10^7 Msunclusters near the inner Lindblad resonance of the barred spiral NGC 1365. Themorphology, mass, and flow of HI and CO gas in the spiral and barred regionsare examined for evidence of the location and mechanism of cluster formation.The accretion rate is compared with the star formation rate to infer thelifetime of the starburst. The gas appears to move from inside corotation inthe spiral region to looping filaments in the interbar region at a rate of ~6Msun/yr before impacting the bar dustlane somewhere along its length. The gasin this dustlane moves inward, growing in flux as a result of the accretion to~40 Msun/yr near the ILR. This inner rate exceeds the current nuclear starformation rate by a factor of 4, suggesting continued buildup of nuclear massfor another ~0.5 Gyr. The bar may be only 1-2 Gyr old. Extrapolating the barflow back in time, we infer that the clusters formed in the bar dustlaneoutside the central dust ring at a position where an interbar filamentcurrently impacts the lane. The ram pressure from this impact is comparable tothe pressure in the bar dustlane, and both are comparable to the pressure inthe massive clusters. Impact triggering is suggested. The isothermal assumptionin numerical simulations seems inappropriate for the rare fraction parts ofspiral and bar gas flows. The clusters have enough lower-mass counterparts tosuggest they are part of a normal power law mass distribution. Gas trapping inthe most massive clusters could explain their [NeII] emission, which is notevident from the lower-mass clusters nearby.

Massive Clusters in the Inner Regions of NGC 1365: Cluster Formation and Gas Dynamics in Galactic Bars