We present detailed parameter determinations of two chemically normal late A-type stars, HD 32115 and HD 37594, to uncover the reasons behind large discrepancies between two previous analyses of these stars performed with a semi-automatic procedure and a 'classical' analysis. Our study is based on high-resolution, high signal-to-noise ratio spectra obtained at the McDonald Observatory. Our method is based on the simultaneous use of all available observables: multicolour photometry, pressure-sensitive magnesium lines, metallic lines and Balmer line profiles. Our final set of fundamental parameters fits, within the error bars, all available observables. It differs from the published results obtained with a semi-automatic procedure.