  The aim of our study is to investigate the physical properties of the
star-forming interstellar medium (ISM) in the Large Magellanic Cloud (LMC) by
separating the origin of the emission lines spatially and spectrally. Following
Okada et al. (2015, Paper I), we investigate different phases of the ISM traced
by carbon-bearing species in four star-forming regions in the LMC, and model
the physical properties using the KOSMA-tau PDR model. We mapped 3--13
arcmin$^2$ areas in 30 Dor, N158, N160 and N159 along the molecular ridge of
the LMC in [CII]158um with GREAT on board SOFIA, and in CO(2-1) to (6-5),
$^{13}$CO(2-1) and (3-2), [CI]3P1-3P0 and 3P2-3P1 with APEX. In all four
star-forming regions, the line profiles of CO, $^{13}$CO, and [CI] emission are
similar, whereas [CII] typically shows wider line profiles or an additional
velocity component. For selected positions in N159 and 30 Dor, we observed the
velocity-resolved [OI] 145um and 63um lines for the first time with upGREAT. At
some positions, the [OI] line profiles match those of CO, at other positions
they are more similar to the [CII] profiles. We interpret the different line
profiles of CO, [CII] and [OI] as contributions from spatially separated clouds
and/or clouds in different physical phases, which give different line ratios
depending on their physical properties. We model the emission from the CO,
[CI], [CII], and [OI] lines and the far-infrared continuum emission using the
latest KOSMA-tau PDR model, which treats the dust-related physics consistently
and computes the dust continuum SED together with the line emission of the
chemical species. We find that the line and continuum emissions are not
well-reproduced by a single clump ensemble. Toward the CO peak at N159~W, we
propose a scenario that the CO, [CII], and [OI] 63um emission are weaker than
expected because of mutual shielding among clumps. (abridged for arXiv)
