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We present results obtained towards the HII regions N159, N166, and N132 fromthe emission of several molecular lines in the 345 GHz window. Using ASTE wemapped a 2.4' $\times$ 2.4' region towards the molecular cloud N159-W in the$^{13}$CO J=3-2 line and observed several molecular lines at an IR peak veryclose to a massive young stellar object. $^{12}$CO and $^{13}$CO J=3-2 wereobserved towards two positions in N166 and one position in N132. The $^{13}$COJ=3-2 map of the N159-W cloud shows that the molecular peak is shiftedsouthwest compared to the peak of the IR emission. Towards the IR peak wedetected emission from HCN, HNC, HCO$^{+}$, C$_{2}$H J=4-3, CS J=7-6, andtentatively C$^{18}$O J=3-2. This is the first reported detection of thesemolecular lines in N159-W. The analysis of the C$_{2}$H line yields moreevidence supporting that the chemistry involving this molecular species incompact and/or UCHII regions in the LMC should be similar to that in Galacticones. A non-LTE study of the CO emission suggests the presence of both cool andwarm gas in the analysed region. The same analysis for the CS, HCO$^{+}$, HCN,and HNC shows that it is very likely that their emissions arise mainly fromwarm gas with a density between $5 \times 10^5$ to some $10^6$ cm$^{-3}$. Theobtained HCN/HNC abundance ratio greater than 1 is compatible with warm gas andwith an star-forming scenario. From the analysis of the molecular linesobserved towards N132 and N166 we propose that both regions should have similarphysical conditions, with densities of about 10$^3$ cm$^{-3}$.

A view of Large Magellanic Cloud HII regions N159, N132, and N166 through the 345 GHz window