We study the direct gas-phase oxygen abundance using the well-detected auroral line [ \ion O3 ] \lambda 4363 in the stacked spectra of a sample of local analogs of high-redshift galaxies . These local analogs share the same location as z \sim 2 star-forming galaxies on the [ \ion O3 ] \lambda 5007/H \beta versus [ \ion N2 ] \lambda 6584/H \alpha Baldwin-Phillips-Terlevich diagram . This type of analog has the same ionized interstellar medium ( ISM ) properties as high-redshift galaxies . We establish empirical metallicity calibrations between the direct gas-phase oxygen abundances ( 7.8 < 12 + \log ( O / H ) < 8.4 ) and the N2 ( \log ( [ \ion N2 ] \lambda 6584/H \alpha ) ) /O3N2 ( \log ( ( [ \ion O3 ] \lambda 5007/H \beta ) / ( [ \ion N2 ] \lambda 6584/H \alpha ) ) ) indices in our local analogs . We find significant systematic offsets between the metallicity calibrations for our local analogs of high-redshift galaxies and those derived from the local \ion H2 regions and a sample of local reference galaxies selected from the Sloan Digital Sky Survey ( SDSS ) . The N2 and O3N2 metallicities will be underestimated by 0.05-0.1 dex relative to our calibration , if one simply applies the local metallicity calibration in previous studies to high-redshift galaxies . Local metallicity calibrations also cause discrepancies of metallicity measurements in high-redshift galaxies using the N2 and O3N2 indicators . In contrast , our new calibrations produce consistent metallicities between these two indicators . We also derive metallicity calibrations for R23 ( \log ( ( [ \ion O3 ] \lambda \lambda 4959,5007+ [ \ion O2 ] \lambda \lambda 3726,3729 ) /H \beta ) ) , O32 ( \log ( [ \ion O3 ] \lambda \lambda 4959,5007/ [ \ion O2 ] \lambda \lambda 3726,3729 ) ) , \log ( [ \ion O3 ] \lambda 5007/H \beta ) , and \log ( [ \ion Ne3 ] \lambda 3869/ [ \ion O2 ] \lambda 3727 ) indices in our local analogs , which show significant offset compared to those in the SDSS reference galaxies . By comparing with MAPPINGS photoionization models , the different empirical metallicity calibration relations in the local analogs and the SDSS reference galaxies can be shown to be primarily due to the change of ionized ISM conditions . Assuming that temperature structure variations are minimal and ISM conditions do not change dramatically from z \sim 2 to z \sim 5 , these empirical calibrations can be used to measure relative metallicities in galaxies with the redshifts up to z \sim 5.0 in ground-based observations .