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Hinge clumps are luminous knots of star formation near the base of tidalfeatures in some interacting galaxies. We use archival Hubble Space TelescopeUV/optical/IR images and Chandra X-ray maps along with GALEX UV, Spitzer IR,and ground-based optical/near-IR images to investigate the star formingproperties in a sample of 12 hinge clumps in five interacting galaxies. Themost extreme of these hinge clumps have star formation rates of 1 - 9M(sun)/yr, comparable to or larger than the `overlap' region of intense starformation between the two disks of the colliding galaxy system the Antennae. Inthe HST images, we have found remarkably large (~70 pc) and luminous (M(I) ~12.2 to -16.5) sources at the centers of these hinge clumps, sometimes embeddedin a linear ridge of fainter star clusters. We have found strong X-ray emissionfrom several of these hinge clumps. In most cases, this emission iswell-resolved with Chandra and has a thermal X-ray spectrum, thus it is likelydue to hot gas associated with the star formation. The ratio of theextinction-corrected diffuse X-ray luminosity to the mechanical energy rate(the X-ray production efficiency) for the hinge clumps is similar to that inthe Antennae galaxies, but higher than those for regions in the normal spiralgalaxy NGC 2403. Two of the hinge clumps have point-like X-ray emission muchbrighter than expected for hot gas; these sources are likely `ultra-luminousX-ray sources' (ULXs) due to accretion disks around black holes. The mostextreme of these sources, in Arp 240, has a hard X-ray spectrum and an absorbedX-ray luminosity of ~2 X 10^41 erg/s; more than expected by single high massX-ray binaries (HMXBs), thus it may be either a collection of HMXBs or anintermediate-mass black hole (>=80 M(sun)). [ abridged ]

Extra-Nuclear Starbursts: Young Luminous Hinge Clumps in Interacting Galaxies