This computational tool was described and used in article Rosa Oliveira, R.A., da Silva Oliveira, M.W., Ojeda-González, A., Pillat, V.G., Echer, E., Nieves-Chinchilla T. Resolving the ambiguity of magnetic cloud’s orientation caused by MVA comparing it with a force free model Solar Physics, 2021 (in revision). The authors indicate that this article be cited when the tool is used. This tool aims to incorporate an algebraic and computational method for calculating the angles of the magnetic clouds (MC) axis from the minimum variance analysis (MVA) and correcting them compared to a simulated model from a linear force-free approximation. Consequently, it determines the type of flux rope consistently and automatically. In general, MC measured in situ at 1 Astronomical Unit (AU) may be approximated to have a cylindrical geometry and the internal magnetic field topology is traditionally described by a force free equilibrium flux rope model. The data analyzed in our research were obtained by the Advanced Composition Explorer (ACE) using 64-second averaged interplanetary magnetic field (IMF) and solar wind ion data from the Magnetic Field Experiment (MAG and Solar Wind Electron, Proton, and Alpha Monitor (SWEPAM)), respectively. We used the IMF components, Bx, By, Bz (in geocentric solar ecliptic (GSE) coordinates from the Magnetometer instrument); and the parameters Proton Density np in cm-3), Radial Component of Proton Temperature (TP in Kelvin), the Ratio of alphas/protons (nHe/nP), Proton Speed (VP in km/s). The plasma betap graphs and the latitudinal BLat and longitudinal BLon vector components are calculated from these data. The files made available are executables for operating systems Windows and Linux (tested (Ubuntu)), as well as a data file to replicate some results published in the article referenced above.