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We have carried out a molecular line survey of the candidate massiveprotostar IRAS 23385+6053, covering a 27.2 GHz frequency range in the 330--360GHz atmospheric window. We detected 27 lines originating from a total of 11species.Over a third of the identified molecular lines are from the asymmetrictop molecule methanol (CH$_{3}$OH). We did not detect any emission fromhigh-excitation lines or typical hot core tracers (e.g. CH$_{3}$CN,HCOOCH$_{3}$). We derive a rotation temperature and column density from themethanol emission and estimate lower limits to the beam-averaged column densityof the remaining lines. Upper limits to the beam-averaged column density ofselected species were determined from the non-detection of their rotationlines. We rule out the presence of a hot molecular core associated with IRAS23385+6053 by a combination of the non-detection of CH$_{3}$CN emission and asimple bolometric luminosity approach. The molecular inventory and chemistry ofIRAS 23385+6053 are contrasted to that of more evolved massive star-formingregions and the abundances predicted by recent time-dependent chemical models.The physical and chemical nature of IRAS 23385+6053 is shown to be consistentwith that immediately prior to the hot molecular core stage.Comment: 13 pages, accepted by A&A 21 May 2003. Revised version 13/06/2003  corrects typo in equation

A molecular line survey of the candidate massive Class 0 protostar IRAS 23385+6053