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We have mapped four selected about 0.5 deg x 0.5 deg-sized fields containingSpitzer 8-micron dark regions with APEX/LABOCA at 870 micron. Selectedpositions in the fields were observed in C17O(2-1) to obtain kinematicinformation. The obtained LABOCA maps are used in conjunction with the SpitzerIR images. The total number of clumps identified in this survey is 91, out ofwhich 40 (44%) appear dark at 8 and 24 micron. The remaining clumps areassociated with mid-IR emission. Many of the identified clumps are massiveenough to allow high-mass star formation, and some of them already show clearsignposts of that. Seven clumps associated with extended-like 4.5 micronemission are candidate extended green objects (EGOs). Filamentary dust "ridges"were found towards the Spitzer bubbles N10/11 in one of our fields, whichconforms to the triggered high-mass star formation in the system. The relativenumber of IR-dark and IR-bright clumps suggest that the duration of the formerstage is about 1.6x10^5 yr. The mass distribution of the total sample ofclumps, and that separately constructed for the IR-dark and IR-bright clumps,could be fitted at the high-mass end with the power-law function dN/dlogM ~M^(-0.8...-0.7). The C17O observation positions appear to be dominated bynon-thermal motions, and the data also revealed some potential sites of strongCO depletion. In G11.36+0.80, which is the best example of a filamentary IRDCin our sample, the clumps appear to be gravitationally bound. The fragmentationof the filament can be understood in terms of a "sausage"-type fluidinstability, in agreement with the results for other IRDCs. The formation offilamentary IRDCs might be caused by converging turbulent flows, and the sameprocess may play a role in exciting the fluid perturbations responsible for thefragmentation of the clouds into clumps.

LABOCA 870 micron dust continuum mapping of selected infrared-dark cloud regions in the Galactic plane