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This paper presents new images and spectroscopy of NGC 34 (Mrk 938) obtainedwith the du Pont 2.5-m and Baade 6.5-m telescopes at Las Campanas, plusphotometry of an HST archival V image. This Mv = -21.6 galaxy has often beenclassified as a Seyfert 2, yet recently published infrared spectra suggest adominant central starburst. We find that the galaxy features a single nucleus,a main spheroid containing a blue central disk, and tidal tails indicative oftwo former disk galaxies. These galaxies appear to have completed merging. Theremnant shows three clear optical signs that the merger was gas-rich ("wet")and accompanied by a starburst: (1) It sports a rich system of young starclusters, of which 87 have absolute magnitudes -10.0 > Mv > -15.4. Fiveclusters with available spectra have ages in the range 0.1-1.0 Gyr, photometricmasses between 2x10^6 and 2x10^7 Msun, and are gravitationally bound youngglobulars. (2) The blue central disk appears to be young. It is exponential,can be traced to >10 kpc radius, and has a smooth structure and colors suggest-ing a dominant, ~400 Myr old poststarburst population. And (3), the center ofNGC 34 drives a strong outflow of cool, neutral gas, as revealed by broadblueshifted Na I D lines. The mean outflow velocity of this gas is -620 km/s,while the maximum velocity reaches -1050 km/s. We suggest that NGC 34 stemsfrom two recently merged gas-rich disk galaxies with an estimated mass ratiobetween 1/3 and 2/3. The remnant seems to have first experienced a galaxy-widestarburst that then shrank to its current central and obscured state. Thestrong gaseous outflow came last. (Abridged)Comment: 26 pages, 18 figures, 8 tables (emulateapj). Accepted for publication  in The Astronomical Journal, Vol. 133. Figs. 1, 2, 3, & 5 degraded to reduce  file size

Remnant of a "Wet" Merger: NGC 34 and Its Young Massive Clusters, Young Stellar Disk, and Strong Gaseous Outflow