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There are only a few ``dark galaxy'' candidates discovered to date in thelocal Universe. One of the most prominent of them is the SW component of amerging system HI 1225+01. On the other hand, the number of known verymetal-poor gas-rich dwarfs similar to IZw18 and SBS 0335-052 E,W has growndrastically during the last decade, from a dozen and a half to about fivedozen. Many of them are very gas-rich, having from ~90 to 99% of all baryons ingas. For some of such objects that have the deep photometry data, no evidencesfor the light of old stars are found. At least a half of such galaxies with theprominent starbursts have various evidences of interactions, including advancedmergers. This suggests that a fraction of this group objects can be a kind ofvery stable protogalaxies (or ``dark galaxies''), which have recentlyexperienced strong disturbances from nearby massive galaxy-size bodies. Such acollision caused the gas instabilities and its collapse with the subsequentonset of starburst. We briefly discuss the morphology and gas kinematics forthe subsample of the most metal-poor dwarfs that illustrate this picture. Wediscuss also the relation of these rare galaxies to the processes by which``dark galaxies'' can occasionally transform to optically visible galaxies.

"Dark galaxies" and local very metal-poor gas-rich galaxies: possible interrelations